HCO + Imaging of Comet C/Hale-Bopp 1995 O1

Details HCO + Imaging of Comet C/Hale-Bopp 1995 O1 HCO + Imaging of Comet C/Hale-Bopp 1995 O1

Apr 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...497l.117l&link_type=abstract

Astrophysical Journal Letters v.497, p.L117

Astronomy and Astrophysics

Astronomy

16

Comets: Individual Name: Hale-Bopp 1995 O1, Molecular Processes, Plasmas, Radio Lines: Solar System

Scientific paper

The HCO ^{+} J=1-0 rotational transition at 89.189 GHz has been mapped in comet Hale-Bopp (C/1995 O1) over a total of 38 individual days spanning the period 1997 March 10-June 20 with the Five College Radio Astronomy Observatory 14 m antenna. HCO ^{+} is detectable over an extended region of the comet, with the peak emission commonly located 50,000-100,000 km in the antisolar direction. Maps made throughout the apparition show significant variability in the structure of the HCO ^{+} coma, sometimes on timescales of several hours. The HCO ^{+} brightness is usually depressed at the nucleus position, and on some occasions, the emission is spread into a ring around the position of the nucleus. Individual spectra within the maps display broad (approximately 4 km s ^{-1} ) lines redshifted by 1-2 km s ^{-1} or more from the nominal velocity of the nucleus, with the redshift typically increasing in the antisolar direction. The spectra and maps may be generally explained by models in which the ions are accelerated tailward at a rate on the order of 10 cm s ^{-2} , provided that HCO ^{+} is destroyed within 50,000-100,000 km of the nucleus.

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